We restrict the radial extent of the
line-of-sight velocity dispersion profiles to the same range for which we have proper motion dispersions in order to avoid a possible bias due to the \(N\) -body models not providing a
match to the full profile. In the \(N\) -body models we measure the line-of-sight velocity dispersion profile for stars brighter than the main-sequence turnoff. The magnitude limit
for the proper motion velocity dispersion profiles was varied for each data set independently so we match the magnitude limit of the observed data. Hence, except for the nearest clusters like NGC 6121,
we chose a magnitude limit equal to the main-sequence turnoff for fits to the Gaia EDR3 proper motions, while we choose deeper limits for the HST data. The left and middle panels of Fig. REF 
show the resulting fits to two clusters that have both Gaia and HST data
and Table REF  gives the derived distances from the HST data together with the kinematic distances derived by the authors of the original papers. There is usually good agreement
between the distances derived by us and the original kinematic distances. The only exceptions are NGC 5904 and NGC 6266. At least for NGC 5904, one the reason for different distances could be
the lack of a radial overlap between the line-of-sight and proper motion velocity dispersion profiles used by [1]}, which makes the derived distance strongly dependent on the
dynamical model used for the cluster.
